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Rotating Neutron Stars

Phil Rosenfield, Fridolin Weber, Horst Lenske. Rotating Neutron Stars. Outline. Neutron stars: a short synopsis The structure of neutron stars Modeling neutron stars The equation of state Rotating or non-rotating Two results Conclusions. Introduction.

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Rotating Neutron Stars

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  1. Phil Rosenfield, Fridolin Weber, Horst Lenske Rotating Neutron Stars

  2. Outline • Neutron stars: a short synopsis • The structure of neutron stars • Modeling neutron stars • The equation of state • Rotating or non-rotating • Two results • Conclusions

  3. Introduction A neutron star is left over from the supernova of a star not massive enough to leave a black hole.

  4. Introduction • Mass: 1-2 MSun • Radius: 10 - 15 km • Huge magnetic fields • Extremely dense • Fastest Rotation Rate: 1122 Hz • 107−9 in a typical galaxy Objects that don’t make sense, thatcan’t be explained with current theories, are the guides thatlead us to better understanding our universe. If I could get my bike tires going that fast, I’d be moving at 1,700mph. On the surface of a typical sized neutron star, particles aremoving at 80%c!

  5. The structure of neutron stars

  6. Modeling Neutron Stars Non Rotating Rotating Poles shrink, equator bulges Maximum rotation rate Frame dragging • Spherically Symmetric • Curved space-time

  7. Results Mass-Equatorial Radius Period-Mass Rotation  More mass • Rotation  Larger Radius

  8. Conclusions • Rotation matters • These equations of state can explain the fastest spinning neutron stars What’s Next Going to grad school – hope to look for more neutron stars

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